deletions | additions       diff --git a/Magnetic Trapping.tex b/Magnetic Trapping.tex  index 06afc6b..21c9da5 100644  --- a/Magnetic Trapping.tex  +++ b/Magnetic Trapping.tex 
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Let's now look at magneto-gravity waves that are reflected at $r_{\rm MG}$. These waves do not couple directly to Alfven modes. However, as the reflecting boundary can not be spherically symmetric (since $\nabla \cdot \textbf{B} = 0$) and purely poloidal fields are unstable, the incoming $\ell=1$ wave is also scattered into higher $\ell$ modes. Similarly to pure Alfven modes, these waves can not couple back to acoustic modes in the envelope, their tunneling integral being very large.   Therefore they are also effectively trapped in the magneto-gravity cavity.   We have shown that, due to the magnetic greenhouse effect, waves that make it through the evanescent region can not escape from a magnetized stellar core. The Since for $\ell=1$ modes the mode inertia in the core is usually comparable to the mode inertia in the acoustic cavity, one expects that their  degree of suppressionof any modes visible at the surface  istherefore  largely controlled by the degree of reflection at the bottom of the acoustic cavity, as cavity (as  determined by the tunneling integral through the evanescent region (See Eq.~\reg{eqn:integral} region, see Eq.~\ref{eqn:integral}  and Fig.~\ref{visibility}).